Qatar-1

Last updated
Qatar-1
Observation data
Epoch J2000       Equinox
Constellation Draco
Right ascension 20h 13m 31.6176s
Declination 65° 09′ 43.4909″
Apparent magnitude  (V)12.84
Characteristics
Evolutionary stage main sequence star
Spectral type K3V
B−V color index 1.06
V−R color index 0.19
J−H color index 0.472
J−K color index 0.590
Variable type planetary transit variable
Astrometry
Radial velocity (Rv)-37.835±0.063 km/s
Proper motion (μ)RA: 12.636±0.048  mas/yr
Dec.: 58.170±0.041  mas/yr
Parallax (π)5.3587 ± 0.0231  mas
Distance 609 ± 3  ly
(186.6 ± 0.8  pc)
Details [1] [2]
Mass 0.85±0.03  M☉
Radius 0.823±0.025  R☉
Surface gravity (log g)4.536±0.024  cgs
Temperature 4861±125  K
Metallicity [Fe/H]0.2±0.1  dex
Rotational velocity (v sin i)1.7±0.3 km/s
Age 4.5  Gyr
Other designations
Qatar-1, 2MASS J20133160+6509433, Gaia DR2 2244830490514284928, V592 Dra [3]
Database references
SIMBAD data

Qatar-1 is an orange main sequence star in the constellation of Draco.

Contents

Star characteristics

Qatar-1 has an average to high metallicity of 160% of solar, [1] and is of similar age to Sun. [2] The star has significant starspot activity. [4]

Planetary system

The "Hot Jupiter" class planet Qatar-1b was discovered by the Qatar Exoplanet Survey in 2010. [1] The planetary orbit is likely aligned with the rotational axis of the star, with the misalignment measurement based on the Rossiter-McLaughlin effect equal to −8.4±7.1 degrees. [2] The planet has a large measured temperature difference between dayside (1696±39 K) and nightside (1098±158 K). [5] A spectroscopic study in 2017 does suggest that Qatar-1b has relatively clear skies with a few clouds. [6]

Additional planets or a brown dwarf in the system were suspected in 2013, [7] but were refuted in 2015. [8] [9]

The transit-timing variation search in 2020 has also resulted in no detection of additional planets in the system, [10] [11] although by 2022 additional transit-timing variation data have suggested the planetary system is accelerating under influence of the unseen long-period companion. [12]

The Qatar-1 planetary system [1] [2] [10]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b1.33±0.05  MJ 0.02343±0.00121.4200236±0.0000001 [11] 0.020+0.011
−0.01		84.23±0.06° 1.19±0.09  RJ

Related Research Articles

<span class="mw-page-title-main">TrES-3b</span>

TrES-3b is an extrasolar planet orbiting the star GSC 03089-00929. It has an orbital period of just 31 hours and nearly twice the mass of Jupiter.

<span class="mw-page-title-main">WASP-4</span> G-type main sequence star in the constellation Phoenix

WASP-4 is a G-type main sequence star approximately 891 light-years away in the constellation of Phoenix. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by a giant planet on close orbit.

GSC 03089-00929 is a magnitude 12 star located approximately 760 light-years away in the constellation of Hercules. This star is a G type main sequence star that is similar to but slightly cooler than the Sun. This star is identified in SIMBAD as a variable star per the 1SWASP survey.

HAT-P-12 is a magnitude 13 low-metallicity K dwarf star approximately 463 light years away in the constellation Canes Venatici, which hosts one known exoplanet.

<span class="mw-page-title-main">Kepler-27</span> G-type star in the constellation Cygnus

Kepler-27 is a star in the northern constellation of Cygnus, the swan. It is located at the celestial coordinates: Right Ascension 19h 28m 56.81962s, Declination +41° 05′ 09.1405″. With an apparent visual magnitude of 15.855, this star is too faint to be seen with the naked eye.

Kepler-51 is a Sun-like star that is about 500 million years old. It is orbited by three super-puff planets—Kepler-51b, c, and d—which have the lowest known densities of any known exoplanet. The planets are similar in radius to gas giants like Jupiter, but have unusually small masses for their size, only a few times greater than Earth’s.

HAT-P-26 is a K-type main-sequence star about 466 light-years away. A survey in 2015 did not find any stellar companions in orbit around it, although a red dwarf companion with a temperature 4000+100
−350 K is suspected on wide orbit.

WASP-46 is a G-type main-sequence star about 1,210 light-years away. The star is older than the Sun and is strongly depleted in heavy elements compared to the Sun, having just 45% of the solar abundance. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by a giant planet on a close orbit.

Qatar-2 is a K-type main-sequence star about 595 light-years away in the constellation of Virgo. The star is much older than Sun, and has a concentration of heavy elements similar to solar abundance. The star features a numerous and long-lived starspots, and belongs to a peculiar variety of inflated K-dwarfs with strong magnetic activity inhibiting internal convection.

WASP-52 is a K-type main-sequence star about 570 light-years away. It is older than the Sun at 10.7+1.9
−4.5 billion years, but it has a similar fraction of heavy elements. The star has prominent starspot activity, with 3% to 14% of the stellar surface covered by areas 575±150 K cooler than the rest of the photosphere.

HD 175289 is a binary star system. Its primary star, also known as Kepler-410A, is a F-type subgiant star, orbited by the orange dwarf star Kepler-410B on a wide orbit. The companion star was discovered in 2012.

References

  1. 1 2 3 4 Alsubai, K. A.; Parley, N. R.; Bramich, D. M.; West, R. G.; Sorensen, P. M.; Collier Cameron, A.; Latham, D. W.; Horne, K.; Anderson, D. R.; Bakos, G. Á.; Brown, D. J. A.; Buchhave, L. A.; Esquerdo, G. A.; Everett, M. E.; Fűrész, G.; Hartman, J. D.; Hellier, C.; Miller, G. M.; Pollacco, D.; Quinn, S. N.; Smith, J. C.; Stefanik, R. P.; Szentgyorgyi, A. (2011). "Qatar-1b: A hot Jupiter orbiting a metal-rich K dwarf star". Monthly Notices of the Royal Astronomical Society. 417 (1): 709–716. arXiv: 1012.3027 . Bibcode:2011MNRAS.417..709A. doi:10.1111/j.1365-2966.2011.19316.x. S2CID   55675165.
  2. 1 2 3 4 Covino, E.; Esposito, M.; Barbieri, M.; Mancini, L.; Nascimbeni, V.; Claudi, R.; Desidera, S.; Gratton, R.; Lanza, A. F.; Sozzetti, A.; Biazzo, K.; Affer, L.; Gandolfi, D.; Munari, U.; Pagano, I.; Bonomo, A. S.; Collier Cameron, A.; Hébrard, G.; Maggio, A.; Messina, S.; Micela, G.; Molinari, E.; Pepe, F.; Piotto, G.; Ribas, I.; Santos, N. C.; Southworth, J.; Shkolnik, E.; Triaud, A. H. M. J.; et al. (2013). "The GAPS programme with HARPS-N at TNG". Astronomy & Astrophysics. 554: A28. arXiv: 1304.0005 . doi:10.1051/0004-6361/201321298. S2CID   54793301.
  3. ↑ Qatar 1 -- High proper-motion Star
  4. ↑ Mislis, D.; Mancini, L.; Tregloan-Reed, J.; Ciceri, S.; Southworth, J.; d'Ago, G.; Bruni, I.; Baştürk, Ö.; Alsubai, K. A.; Bachelet, E.; Bramich, D. M.; Henning, Th.; Hinse, T. C.; Iannella, A. L.; Parley, N.; Schroeder, T. (2015). "High-precision multiband time series photometry of exoplanets Qatar-1b and TrES-5b". Monthly Notices of the Royal Astronomical Society. 448 (3): 2617–2623. arXiv: 1503.02246 . Bibcode:2015MNRAS.448.2617M. doi:10.1093/mnras/stv197. S2CID   53561305.
  5. ↑ May, Erin; Stevenson, Kevin; Bean, Jacob; Bell, Taylor; Cowan, Nicolas; Dang, Lisa; Desert, Jean-Michel; Fortney, Jonathan; Keating, Dylan; Kempton, Eliza; Komacek, Thaddeus; Lewis, Nikole; Mansfield, Megan; Morley, Caroline; Parmentier, Vivien; Rauscher, Emily; Swain, Mark; Zellem, Robert; Showman, Adam (2022), "A New Analysis of Eight Spitzer Phase Curves and Hot Jupiter Population Trends: Qatar-1b, Qatar-2b, WASP-52b, WASP-34b, and WASP-140b", The Astronomical Journal, 163 (6): 256, arXiv: 2203.15059 , Bibcode:2022AJ....163..256M, doi: 10.3847/1538-3881/ac6261 , S2CID   247778438
  6. ↑ von Essen, C.; Cellone, S.; Mallonn, M.; Albrecht, S.; Miculán, R.; Müller, H. M. (2017). "Testing connections between exo-atmospheres and their host stars". Astronomy & Astrophysics. 603: A20. arXiv: 1703.10647 . doi:10.1051/0004-6361/201730506. S2CID   119452420.
  7. ↑ von Essen, C.; Schröter, S.; Agol, E.; Schmitt, J. H. M. M. (2013). "Qatar-1: Indications for possible transit timing variations". Astronomy & Astrophysics. 555: A92. arXiv: 1309.1457 . Bibcode:2013A&A...555A..92V. doi:10.1051/0004-6361/201321407. S2CID   119174903.
  8. ↑ MacIejewski, G.; Fernández, M.; Aceituno, F. J.; Ohlert, J.; Puchalski, D.; Dimitrov, D.; Seeliger, M.; Kitze, M.; Raetz, St.; Errmann, R.; Gilbert, H.; Pannicke, A.; Schmidt, J.-G.; Neuhäuser, R. (2015). "No variations in transit times for Qatar-1 B". Astronomy & Astrophysics. 577: A109. arXiv: 1503.07191 . Bibcode:2015A&A...577A.109M. doi:10.1051/0004-6361/201526031. S2CID   118638934.
  9. ↑ Collins, Karen A.; Kielkopf, John F.; Stassun, Keivan G. (2015). "TRANSIT TIMING VARIATION MEASUREMENTS OF WASP-12b AND QATAR-1b: NO EVIDENCE OF ADDITIONAL PLANETS". The Astronomical Journal. 153 (2): 78. arXiv: 1512.00464 . doi: 10.3847/1538-3881/153/2/78 . S2CID   55191644.
  10. 1 2 Thakur, Parijat; Mannaday, Vineet Kumar; Sahu, Devendra Kumar; Chand, Swadesh; Jiang, Ing-Guey (2020), "Investigating Extra-solar Planetary System Qatar-1 through Transit Observations", Bulletin de la Société Royale des Sciences de Liège: 132–136, arXiv: 2007.03753 , doi:10.25518/0037-9565.7577, S2CID   54660279
  11. 1 2 Su, Li-Hsin; Jiang, Ing-Guey; Sariya, Devesh P.; Lee, Chiao-Yu; Yeh, Li-Chin; Mannaday, Vineet Kumar; Thakur, Parijat; Sahu, D. K.; Chand, Swadesh; Shlyapnikov, A. A.; Moskvin, V. V.; Ignatov, Vladimir; Mkrtichian, David; Griv, Evgeny (2021), "Are There Transit Timing Variations for the Exoplanet Qatar-1b?", The Astronomical Journal, 161 (3): 108, arXiv: 2012.08184 , Bibcode:2021AJ....161..108S, doi: 10.3847/1538-3881/abd4d8 , S2CID   229181287
  12. ↑ Mannaday, Vineet Kumar; Thakur, Parijat; Southworth, John; Jiang, Ing-Guey; Sahu, D. K.; Mancini, L.; Vaňko, M.; Kundra, Emil; Gajdoš, Pavol; a-Thano, Napaporn; Sariya, Devesh P.; Yeh, Li-Chin; Griv, Evgeny; Mkrtichian, David; Shlyapnikov, Aleksey (2022), "Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data", The Astronomical Journal, 164 (5): 198, arXiv: 2209.04080 , Bibcode:2022AJ....164..198M, doi: 10.3847/1538-3881/ac91c2 , S2CID   252185524


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